Figure 3

Two-dimensional simulation of primordial star formation including radiation from the central protostar. The panels shows the temperature and number density of the cloud at various output times. The ionizing radiation clears out the gas along the poles, while the accretion continues nearly unabated in the plane of the disk. As the photo-heated region expands, it shuts down the mass flow from the envelope onto the disk, which eventually terminates accretion. Here, the star reaches a final mass of \({\simeq}40\mbox { M}_{\odot}\). Adapted from Hosokawa et al. (2011).